Turbulently Driven Detonation Initiation in Electron-degenerate Matter with Helium

Abstract

Type Ia supernovae (SNe Ia) are standardizable cosmological candles that led to the discovery of the accelerating Universe. However, the physics of how white dwarfs (WDs) explode and lead to SNe Ia is still poorly understood. The initiation of the detonation front that rapidly disrupts the WD is a crucial element of the puzzle, and global 3D simulations of SNe Ia cannot resolve the requisite length scales to capture detonation initiation. In this work, we elucidate a theoretical criterion for detonation initiation in the distributed burning regime. We test this criterion against local 3D driven turbulent hydrodynamical simulations within electron-degenerate WD matter consisting initially of pure helium. We demonstrate a novel pathway for detonation, in which strong turbulent dissipation rapidly heats the helium, and forms carbon nuclei sufficient to lead to a detonation through accelerated burning via α captures. Simulations of strongly driven turbulent conditions lead to detonations at a mean density of 10 ^6 g cm ^−3 and mean temperature of 1.4–1.8 × 10 ^9 K, but fail to detonate at a lower density of 10 ^5 g cm ^−3 , in excellent agreement with theoretical predictions.

Keywords

• Helium burning
• Astrophysical explosive burning
• Nuclear astrophysics
• Hydrodynamics
• Hydrodynamical simulations